deletions | additions       diff --git a/h2o_megamasers.tex b/h2o_megamasers.tex  index 9407ce4..6731737 100644  --- a/h2o_megamasers.tex  +++ b/h2o_megamasers.tex 
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\item   \end{itemize}  \subsection{Extragalactic versus Galactic Mega-maser  Properties} \label{sub:h2o_props}  Galactic  \begin{itemize}  \item   \end{itemize}  Extragalactic  \begin{itemize} 
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\item masers are unique tool to probe ~pc regions around AGN -- other bands are highly obscured  \item characteristically have triple peak in velocity -- center at systematic vel of galaxy, w shifted by hundreds of km/s -- rotation of disk  \item NGC 4258 best studied for this (Miyoshi+95, Herrnstein+99) -- MCP has greatly extended this  \item Disks appear to be thin and keplerian, extending to sub-pc distances from the AGN  \item rotation curves implied by the disk (and the small compact scales involved) give direct measurement of the SMBH masses  \item greene+10 model the maser rotation curves to derive BH masses; use SDSS to derive stellar velocity dispersions -- to very high precision!! (<15\%)  \item find that maser galaxies fall below the $M_BH-\sigma$ relation defined for ellipticals -- the relation cannot be used to derive the BH mass function for AGN -- NO UNIVERSAL power-law MBH-sigma relation  \item Find M_BH relates to properties of the bulge, but not strongly with overall galactic luminosity  \item Combined with full rotation curves of these galaxies (ie from HI), can check for correlation of M_BH w/ mass of dark matter halo (Ferrarese 02, at least for non-spiral galaxies)  \item wardle yusef-zadeh 21 derive a relation b/w MM disk radius and BH mass  \item argue that disks are formed through capture of MCs passing through galactic nucleus (w/in some impact parameter)  \item Find R=4G\lambda^2M/v^2, where \lambda is the fraction of angular momentum reduced when cloud enters the disc, v is cloud velocity, M is BH mass  \item matches observational values  \item greene+13 explore using MM disks to find BH accretion  \item use HST/WFC3 to observ 9 MM disk galaxies; young stars seen, MM disks do not align w/ circumnuclear disks or bars of stars  \item disk preferentially aligned w/ radio continuum jets on up to 50 pc scales  \item ALMA will allow to search the gas component directly at sub-" resolution  \item favour misalignment scenario due to accretion changing angular momentum as a function of scale  \item the misalignment between the 2 components may be related to accretion on the BH -- disk warping from radiation pressure (pringle 97),angular momentum changes w/ scale due to accretion events (hopkins \& quataert 10, 11); disk alignments boost accretion rate (nixon+12) - gas angular momentum dissipated where disks meet, could boost accretion rate by 1 dex; gas from external sources giving accretion at random angles from small satellites  \end{itemize}  \subsection{Jet masers}